[1]}, who assumed
\(f_\mathrm {C}=37.5\)  % and silicate for the rest (see above for the other parameters), used the MieX code [2]} to obtain \(\kappa _{\bullet ,\,\mathrm {H}\,\alpha }=1300\)  cm\(^2\)  g\(_\mathrm {dust}^{-1}\) . With their reference global mass ratio \(f_{\textrm {d/g}}=10^{-2}\) , their opacity as a cross-section per gram of gas fits within our range. The same holds for the opacity of [3]} (see above), which we computed with OpTool to be \(\kappa _{\bullet ,\,\mathrm {H}\,\alpha }=280\)  cm\(^2\)  g\(_\mathrm {dust}^{-1}\) . It is however at the lower edge of the range of intrinsic opacities because of their large maximal grain size (\(a_{\rm max}=3\)  mm). Such large grains are not expected in our case, in the accretion flow onto a growing planet.
